https://doi.org/10.1140/epjc/s10052-025-14596-x
Regular Article - Theoretical Physics
Comprehensive analysis of dark energy stars in R-squared gravity
1
Astrophysics and Cosmology Research Unit, School of Mathematics, Statistics and Computer Science, University of KwaZulu–Natal, Private Bag X54001, 4000, Durban, South Africa
2
Department of Basic Sciences, General Administration of Preparatory Year, King Faisal University, P.O. Box 400, 31982, Al Ahsa, Saudi Arabia
3
Department of Mathematics and Statistics, College of Science, King Faisal University, P.O. Box 400, 31982, Al Ahsa, Saudi Arabia
4
National University of Uzbekistan, 100174, Tashkent, Uzbekistan
5
Tashkent International University of Education, Imom Bukhoriy 6, 100207, Tashkent, Uzbekistan
6
University of Tashkent for Applied Sciences, Str. Gavhar 1, 100149, Tashkent, Uzbekistan
7
Tashkent State Technical University, 100095, Tashkent, Uzbekistan
8
Kimyo International University in Tashkent, Shota Rustaveli Street 156, 100121, Tashkent, Uzbekistan
9
Mamun University, Bolkhovuz Street 2, 220900, Khiva, Uzbekistan
10
Department of Technique, Urgench State University, Kh. Alimjan Str. 14, 221100, Urgench, Uzbekistan
Received:
10
May
2025
Accepted:
28
July
2025
Published online:
5
August
2025
This study examines the structure and stability of dark energy stars within the context of 
gravity, with the gravity model defined by 
(the Starobinsky model). Specifically, dark energy is a mysterious force that can prevent the gravitational collapse of compact objects to singularities. To characterize dark energy, we consider modified Chaplygin fluid as an equation of state (EoS) of matter and study its mass-radius relation for different model parameters. By numerically solving the modified Tolman–Oppenheimer–Volkoff (TOV) equations, our primary objective is to examine the influence of variations in the gravity parameter a on the energy density, pressure, mass-radius and mass-central density relationships of dark energy stars. Our findings reveal that the variation of a does not significantly impact on the 
relations but comfortably exceeds the 2
limit. Additionally, we examine the dynamical stability of these stars by evaluating the static stability criterion, adiabatic index, and sound speed. Finally, we compare our results with various astrophysical observational data and discuss future observations that could validate the predictions of our model.
© The Author(s) 2025
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Funded by SCOAP3.
